Estimation of a Coronal Mass Ejection Magnetic Field Strength using Radio Observations of Gyrosynchrotron Radiation

摘要: Coronal mass ejections (CMEs) are large eruptions of plasma and magnetic field from the low solar corona into interplanetary space. These often associated with acceleration energetic electrons which produce various sources high intensity emission. In relatively rare cases, may also gyrosynchrotron emission within CME itself, allowing for a diagnostic strength. Such is important evaluating total energy content CME, ultimately what drives eruption. Here we report on an unusually source radiation in form type IV radio burst occurring 2014-September-01, observed using instrumentation Nancay Radio Astronomy Facility. A combination spectral flux density measurements instruments Solar Telescope Network (RSTN) 300MHz to 5 GHz reveals spectrum peak at $>$1 GHz. Using this analysis, model radiation, non-thermal electron Fermi Gamma Ray Burst Monitor (GBM) images eruption GOES Soft X-ray Imager (SXI), able calculate both strength properties emitting CME. We find produced by energies >1MeV index $\delta$$\sim$3 4.4 G height 1.3 R$_{\odot}$, while similar distribution but much lower order 10 keV. conclude comparing radio-emitting distributions how such analysis can be used define